VISION – Vienna survey in Orion - III. Young stellar objects in Orion A

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Volume 622 (February 2019)

A&A, 622 (2019) A149

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Table 6.

The MGM YSO sample revisited in numbers.

MGM		This work

		YSOs				False positives^b				Uncertain^c		Total contamination^d

Class	Nr	All^a	P	F	D	Galaxies	Fuzz	MS/III	Artifacts	UG	UY	f.p.	f.p. + U
All	2827	2697 (95.4%)	176	175	2347	37	44	7	4	18	20	92 (3.3%)	130 (4.6%)
D	2442	2376 (97.3%)	10	59	2307	19	26	7	3	–	11	55 (2.3%)	66 (2.7%)
P	330	303 (91.8%)	159	110	34	8	13	–	–	2	4	21 (6.4%)	27 (8.2%)
FP	49	15 (30.6%)	2	7	6	10	4	–	–	15	5	14 (28.6%)	34 (69.4%)
RP	6	3 (50.0%)	3	–	–	–	1	–	1	1	–	2 (33.3%)	3 (50.0%)
P,FP,RP	385	321 (83.4%)	164	117	40	18	18	–	1	18	9	37 (9.6%)	64 (16.6%)

Notes. Shown is the re-classification and proposed contamination (false positives) from this work. Uncertain sources are given separately.

^(a)

The total number of remaining YSO candidates is the sum of the three classes (P, F, D).

^(b)

Different types of false positives: Galaxies, Nebulosities (Fuzz), main-sequence stars or Class III candidates (MS/III), and contamination from image artifacts (C).

^(c)

The number of uncertain objects are given separately for uncertain galaxy candidates (UG), and uncertain YSO candidates (UY).

^(d)

Summarized contamination, giving a lower and upper limit based on the sum of false positives (f.p.) and the sum when including uncertain candidates (f.p. + U).

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